![On the nature of sn stars. I. A detailed abundance study](http://s1.studyres.com/store/data/015532048_1-99b6cf062fdbe46196fe7507ce68a63d-300x300.png)
On the nature of sn stars. I. A detailed abundance study
... and other photometric systems, depending on the chemical peculiarity. For the case of HgMn stars, the Teff directly derived by Strömgren photometry is overestimated, so that a correction is neccessary (Adelman & Rayle 2000; Netopil et al. 2008). We corrected the derived values of the HgMn star HD 23 ...
... and other photometric systems, depending on the chemical peculiarity. For the case of HgMn stars, the Teff directly derived by Strömgren photometry is overestimated, so that a correction is neccessary (Adelman & Rayle 2000; Netopil et al. 2008). We corrected the derived values of the HgMn star HD 23 ...
Celestial Navigation — A Home Study Course
... Introduction to twilight times, sight reduction of all bodies. Read: Chapter 7, Chapter 8, and Chapter 9. You may choose to break this Lesson up into 3 sessions, one for each body, and concentrate on it till it is done. Our work forms are designed to make all sights essentially the same, so in the a ...
... Introduction to twilight times, sight reduction of all bodies. Read: Chapter 7, Chapter 8, and Chapter 9. You may choose to break this Lesson up into 3 sessions, one for each body, and concentrate on it till it is done. Our work forms are designed to make all sights essentially the same, so in the a ...
Star Clusters - Caltech Astronomy
... 35 parsecs, but again there are some in the outer halo with much larger tidal radii. Open clusters Some 1200 open clusters have been catalogued, but as many as 250 of these appear to be simply slight enhancements in the stellar density along a line of sight or small asterisms of unrelated stars. Suc ...
... 35 parsecs, but again there are some in the outer halo with much larger tidal radii. Open clusters Some 1200 open clusters have been catalogued, but as many as 250 of these appear to be simply slight enhancements in the stellar density along a line of sight or small asterisms of unrelated stars. Suc ...
Comprehensive search for natural satellites of Vesta by the Dawn
... SOI with Earth, Jupiter, Ceres, a NEO and Pluto in Table 1. Ceres contains approximately a third of the current asteroid belt by mass (e.g. O’Brien and Sykes, 2011), with Vesta being the second most massive. Vesta has a reasonably-sized SOI relative to other bodies with natural satellites, and if th ...
... SOI with Earth, Jupiter, Ceres, a NEO and Pluto in Table 1. Ceres contains approximately a third of the current asteroid belt by mass (e.g. O’Brien and Sykes, 2011), with Vesta being the second most massive. Vesta has a reasonably-sized SOI relative to other bodies with natural satellites, and if th ...
astro-ph/0303282 PDF
... Since it is highly unlikely that all objects would be planetary companions, by using the brightest object in each field as a reference grid we would expect to measure a change in position equal to the proper motion of the primary star; in fact, within the errors, no candidates changed their relative ...
... Since it is highly unlikely that all objects would be planetary companions, by using the brightest object in each field as a reference grid we would expect to measure a change in position equal to the proper motion of the primary star; in fact, within the errors, no candidates changed their relative ...
Chapter 19
... helium in a processes called nuclear fusion. • The End Stars usually lose material slowly, but sometimes they can lose material in a big explosion. Much of a star’s material returns to space, where it sometimes forms new stars. Chapter menu ...
... helium in a processes called nuclear fusion. • The End Stars usually lose material slowly, but sometimes they can lose material in a big explosion. Much of a star’s material returns to space, where it sometimes forms new stars. Chapter menu ...
Dark Matter, Dark Energy, and the Fate of the Universe
... spherical halo that surrounds the disk of our galaxy, extending to distances well beyond those at which we observe globular clusters and other halo stars. Moreover, the total amount of this mass is more than 10 times the total mass of all the stars in the disk. Because we have detected very little r ...
... spherical halo that surrounds the disk of our galaxy, extending to distances well beyond those at which we observe globular clusters and other halo stars. Moreover, the total amount of this mass is more than 10 times the total mass of all the stars in the disk. Because we have detected very little r ...
the stebbins galaxy: the origins of interstellar medium studies
... 1) The distribution of globular clusters, presumed to be centered around the center of mass of the Galaxy, shows the Sun to be far from that center. 2) The measured distances to globular clusters show the Galaxy to be about 70,000 parsecs (200,000 light-years or so) in diameter (Shapley, 1930a: 221) ...
... 1) The distribution of globular clusters, presumed to be centered around the center of mass of the Galaxy, shows the Sun to be far from that center. 2) The measured distances to globular clusters show the Galaxy to be about 70,000 parsecs (200,000 light-years or so) in diameter (Shapley, 1930a: 221) ...
Review: How does a star`s mass determine its life story?
... • Quantum mechanics says that electrons must move faster as they are squeezed into a very small space. • As a white dwarf’s mass approaches 1.4MSun, its electrons must move at nearly the speed of light. • Because nothing can move faster than light, a white dwarf cannot be more massive than 1.4MSun • ...
... • Quantum mechanics says that electrons must move faster as they are squeezed into a very small space. • As a white dwarf’s mass approaches 1.4MSun, its electrons must move at nearly the speed of light. • Because nothing can move faster than light, a white dwarf cannot be more massive than 1.4MSun • ...
3. The MONS Telescope requirements
... Since the detector is not in focus, a field stop is needed to reject light coming from the field around the target star, which will contain neighbouring stars and background zodiacal light. The field stop also serves to reject scattered light (see below). The diameter of the field stop should be as ...
... Since the detector is not in focus, a field stop is needed to reject light coming from the field around the target star, which will contain neighbouring stars and background zodiacal light. The field stop also serves to reject scattered light (see below). The diameter of the field stop should be as ...
Asteroids - GEOCITIES.ws
... compatriot Johann E. Bode, who used the scheme to advance the notion of a "missing" planet between Mars and Jupiter. The discovery of Uranus in 1781 by the British astronomer William Herschel at a distance that closely fit the distance predicted by Bode's law was taken as strong evidence of its corr ...
... compatriot Johann E. Bode, who used the scheme to advance the notion of a "missing" planet between Mars and Jupiter. The discovery of Uranus in 1781 by the British astronomer William Herschel at a distance that closely fit the distance predicted by Bode's law was taken as strong evidence of its corr ...
Chapter 1 LONG-TERM VARIATIONS IN THE GALACTIC
... Figure 1.3. The history of the SFR. The squares with error bars are the SFR calculated using chromospheric ages of nearby stars (Rocha-Pinto et al., 2000). These data are corrected for different selection biases and are binned into 0.4 Gyr bins. The line and hatched region describe a 1-2-1 average o ...
... Figure 1.3. The history of the SFR. The squares with error bars are the SFR calculated using chromospheric ages of nearby stars (Rocha-Pinto et al., 2000). These data are corrected for different selection biases and are binned into 0.4 Gyr bins. The line and hatched region describe a 1-2-1 average o ...
The white dwarf population within 40 pc of the Sun
... Finally, we mention that the total number of synthetic stars of the restricted samples described below and the observed sample are always similar. In this way we guarantee that the comparison of both sets of data are statistically sound. To produce a consistent white dwarf population, we first gener ...
... Finally, we mention that the total number of synthetic stars of the restricted samples described below and the observed sample are always similar. In this way we guarantee that the comparison of both sets of data are statistically sound. To produce a consistent white dwarf population, we first gener ...
WGCP 5th Jan 16 Astrophotography by Steve Baldwin
... There is a significant list of subjects that fall under the umbrella of astrophotography, not all of them visible after dark: • Lunar images *#% • Starscapes (landscapes taken after dark) and star trails *#% • Milky Way *#% • Planetary conjunctions *#% • ISS and satellites *#% • Meteor showers *# • ...
... There is a significant list of subjects that fall under the umbrella of astrophotography, not all of them visible after dark: • Lunar images *#% • Starscapes (landscapes taken after dark) and star trails *#% • Milky Way *#% • Planetary conjunctions *#% • ISS and satellites *#% • Meteor showers *# • ...
on the pms star hbc 498 and its associated nebulous stars1
... HBC 495 and DL Ori/G2 have Li Iλ6708 Å strong in absorption (see Fig. 2 and Table 3), with equivalent widths stronger than the richest Li I stars with similar spectral types in the Pleiades cluster (i.e., “Li I rich stars”). The Li I line is apparently present in the spectrum of HBC 496, but the sp ...
... HBC 495 and DL Ori/G2 have Li Iλ6708 Å strong in absorption (see Fig. 2 and Table 3), with equivalent widths stronger than the richest Li I stars with similar spectral types in the Pleiades cluster (i.e., “Li I rich stars”). The Li I line is apparently present in the spectrum of HBC 496, but the sp ...
Nebulae.The Lagoon and Dumbbell Nebulae
... is enough to form a star. The remaining matter is supposed to form planets and other planetary objects (moons, asteroids, comets, etc.). ...
... is enough to form a star. The remaining matter is supposed to form planets and other planetary objects (moons, asteroids, comets, etc.). ...
ALMA How does it work and how to use it
... the radio waves coming from the astronomical source at the point known as the focus. The light is reflected by a second reflecting surface –called a subreflector- to a point behind the parabolic surface, where there is a receiver geared to capture the signal concentrated by the antenna. ...
... the radio waves coming from the astronomical source at the point known as the focus. The light is reflected by a second reflecting surface –called a subreflector- to a point behind the parabolic surface, where there is a receiver geared to capture the signal concentrated by the antenna. ...
Earth Centered Universe Pro V6.0
... use one copy of the Software on one computer for use by any one person at a time. You are additionally permitted to install and use the Software on a second computer, provided this second computer is owned by the licensee or used exclusively by the licensee (for example, a notebook computer used in ...
... use one copy of the Software on one computer for use by any one person at a time. You are additionally permitted to install and use the Software on a second computer, provided this second computer is owned by the licensee or used exclusively by the licensee (for example, a notebook computer used in ...
Fast Auto-Focus Method and Software for CCD
... initiated for a ST-8E CCD camera. This value is strongly dependent on how far the star is initially out of focus. Stars farther from focus obviously take longer due to focuser move time and may also require additional exposures. Stars that are not too far from best focus can range between 7th and 1s ...
... initiated for a ST-8E CCD camera. This value is strongly dependent on how far the star is initially out of focus. Stars farther from focus obviously take longer due to focuser move time and may also require additional exposures. Stars that are not too far from best focus can range between 7th and 1s ...
Fast Auto-Focus Method and Software for CCD-based
... to the left shows actual data that was automatically measured on an 8 inch LX-200, ST-8E system during good seeing conditions near sea level. The horizontal axis is the focuser position and the vertical axis is the HFD. This V Curve is an accurate quantitative measure of the telescope optical conver ...
... to the left shows actual data that was automatically measured on an 8 inch LX-200, ST-8E system during good seeing conditions near sea level. The horizontal axis is the focuser position and the vertical axis is the HFD. This V Curve is an accurate quantitative measure of the telescope optical conver ...
The KStars Handbook - KDE Documentation
... examine positional data about the object, and query a huge treasury of online databases for professional-grade astronomical data and literature references about the object. You can even attach your own Internet links, images and text notes, making KStars a graphical front-end to your observing logs ...
... examine positional data about the object, and query a huge treasury of online databases for professional-grade astronomical data and literature references about the object. You can even attach your own Internet links, images and text notes, making KStars a graphical front-end to your observing logs ...
FLARE SWG theme 3: high
... hosts… but less great if lose shorter wavelength (<1.5um), which are required for the rest-frame UV lines. (3) Very few (~5-10) spec-ID’d z>6 quasars from FLARE unless quasars drive the spectroscopic programme (galaxies serendipitiously detected) or have targetted survey. ...
... hosts… but less great if lose shorter wavelength (<1.5um), which are required for the rest-frame UV lines. (3) Very few (~5-10) spec-ID’d z>6 quasars from FLARE unless quasars drive the spectroscopic programme (galaxies serendipitiously detected) or have targetted survey. ...
The Origin and Evolution of Dust in Galaxies
... Dust mass : as a function of metallicity of galaxies It has been suggested that it is difficult to form dust grains in stars in low metallicity (Z<0.1 Z) galaxies But … we found unexpected results ...
... Dust mass : as a function of metallicity of galaxies It has been suggested that it is difficult to form dust grains in stars in low metallicity (Z<0.1 Z) galaxies But … we found unexpected results ...